  We present new photometric observations of the X-ray nova GROJ0422+32 (V518
Per) carried out in the I$_c$ band over 14 nights in 2020 -- 2023. We had to
revise the orbital period of the system, the new value $P_{\rm orb}=5^{\rm
h}04^{\rm m}35.50^{\rm s} \pm 0.04^{\rm s}$ is about one minute shorter than
the period by Webb et al. (2000) but close to the result reported earlier by
Filippenko et al. (1995). The obtained folded light curve has a regular shape
with a clear ellipticity effect and signatures of a slight heating effect. The
simulations of this light curve in terms of the model of an interacting binary
system allowed us to estimate the orbital inclination $i = 33^\circ - 49^\circ$
of the system and derive masses of the black hole $M_x=(6.5\pm2.9)M_\odot$ and
companion star $M_v=(0.47\pm0.21)M_\odot$. This range of the black hole masses
overlaps with the known gap of (2--5)\,M$_\odot$ in the distribution of compact
objects masses but mostly it lies above the upper boundary of this gap. To
obtain more precise estimates one needs to know the degree of heating of the
donor star, so synchronous X-ray/optical observations of this system are
desirable.
