The answer is that the cores of massive stars never become dense enough or centrally concentrated enough to form a black hole during all but the final few seconds of their lives.
The criterion for a (Schwarzschild) black hole is that its mass must be contained within the Schwarzschild radius. The fact that the mass is at the centre of a star is not relevant - the mass surrounding it has no effect.
The Schwarzschild radius is $r_s = 2GM/c^2$. If we write the mass as $M = 4\pi r_s^3\rho/3$, where $\rho$ is a density, then a black hole would be formed if the mass inside $r$
$$ M(r) > \frac{c^2r}{2G}$$
$$ \frac{4\pi}{3}r^3 \rho > \frac{c^2r}{2G}$$
$$\rho > \frac{3c^2}{8\pi G}\left(\frac{1}{r^2}\right)\ .$$
If we put this in sensible stellar units
$$\rho > 3.3\times 10^8 \left(\frac{r}{R_\odot}\right)^{-2}\ {\rm kg}/{\rm m}^3. $$
Thus a black hole would form if the average density within a solar radius was more than 330 million kg/m$^{3}$.
If you want to consider the core of a star (say the inner $0.1R_\odot$), then the density threshold is 100 times higher.
Clearly, the density of the interior of a star cannot grow faster than, or even as fast as $r^{-2}$, otherwise the density would become infinite at the centre.
Thus the answer to your question is that the centres of stars never become dense enough or centrally concentrated enough, except in the late stages of a massive supernova when the core can collapse to $\sim 10^{-5}R_\odot$ amd the density does exceed $3\times 10^{18}$ kg/m$^3$.