Checking for electron degeneracy is a matter of comparing the Fermi kinetic energy with $kT$.
If $E_F/kT \gg 1$, then you may assume the electrons are degenerate.
The central density of the Sun is around $\rho=1.6\times 10^5$ kg/m$^3$ and the number of atomic mass units per electron is around $\mu_e =1.5$.
The number density of electrons is therefore $n_e =\rho/\mu_e m_u = 6.4\times 10^{31}$ m$^{-3}$.
The Fermi momentum is $p_F = (3n_e/8\pi)^{1/3} h = 1.3\times 10^{-23}$ kg m s$^{-1}$. As $p_F \ll m_e c$ then the electrons are non-relativistic and so $E_F \simeq p_F^{2}/2m_e = 9.3\times 10^{-17}$ J.
As the temperature in the solar core is $T =1.57\times 10^7$ K, then $E_F/kT = 0.43$. This ratio is clearly too small for the electrons even to be considered as partially degenerate. (For example, the ratio is more like 1000 in a typical electron-degenerate white dwarf star, and about 20 at the centre of a partially electron-degenerate brown dwarf).
I think this concurs with a treatment based on the de Broglie wavelength. The root of this method is the uncertainty principle in 3D. Degeneracy will be important when
$$(\Delta p \Delta x)^3 \simeq (\hbar/2)^3,$$
where $\Delta x$ is the electron separation and $\Delta p$ is a mean difference in electron momenta.
If we let $\lambda \simeq h/\Delta p$, then we see that degeneracy is important when $\Delta x \simeq \lambda/4\pi$. i.e. Serious degeneracy sets in when the de Broglie wavelength is an order of magnitude greater than the electron separation.
OK, but the ratio isn't zero either, so there will be a small correction to the perfect gas calculation of the pressure. To work this out properly you would have to do a numerical integration to find the pressure due to a very mildly degenerate gas.
To see whether it is worth bothering, you could simply see what the ratio of ideal degeneracy pressure at this electron number density is to the perfect gas pressure in the core of the Sun.
Roughly:
$$ \frac{P_{deg}}{P} = \frac{h^2}{20m_e} \left(\frac{3}{\pi}\right)^{1/3} n_{e}^{5/3} \frac{1}{(n_i +n_e) kT},$$
where $n_i$ is the number density of ions in the gas. If we say $n_i \simeq n_e$ (it's actually a bit smaller because of the helium nuclei present), then put the other numbers in, we find that $P_{deg}/P \sim 0.09$. Thus, I would conclude that if you want to calculate the pressure more accurately than 10 per cent, then you need to take account of the very partial degeneracy of the electrons in the solar core (and its exact composition).
A MUCH more formal treatment (see for example Chapter 2 of Clayton, D. 1983, Principles of Stellar Evolution and Nucleosynthesis, Univ. of Chicago Press), shows that the electron pressure (the ions are non-degenerate and can be treated as a perfect gas) can be written (if the electrons are non-relativistic)
$$ P_{e} = n_e kT \left(\frac{2F_{3/2}}{3F_{1/2}} \right),$$
where the term in the brackets gives the ratio by which the electron gas pressure departs from the perfect gas law, and where
$$F_n(\alpha) = \int_{0}^{\infty} \frac{u^n}{\exp(\alpha + u) + 1}\ du,$$
with $u = E_k/kT$ and $\alpha= -\mu/kT$, where $\mu$ is the chemical potential given by inverting
$$ n_e = \frac{4\pi}{h^3}(2m_e kT)^{3/2} F_{1/2}(\alpha)$$
NB: $\mu \rightarrow E_F$ when $\alpha \ll -1$.
These expressions must be evaluated numerically or taken from tables (e.g. Table 2.3 in Clayton 1983). However, $P_e/n_e kT$ is $\geq 1$ for all values of $\alpha$. So any degeneracy always increases the pressure over that of a perfect gas. The image below (from Clayton 1983) shows how $P_e/n_e kT$ varies with $\alpha$. Clayton says that "the gas pressure is essentially that of a non-degenerate gas for $\alpha>2$".
So putting in some numbers for the Sun, we find $F_{1/2}(\alpha) = 0.19$ and from Table 2.3 of Clayton, we obtain $\alpha \simeq 1.45$. This in turn means that $2F_{3/2}/3 \simeq 0.20$. So the electron pressure is a factor of $\simeq 1.05$ greater than the perfect gas pressure law at the same density and temperature.
