  We simulate numerically the formation of spherically symmetric primordial
black holes (PBHs) seeded by different families of primordial curvature
perturbations profiles on a Friedman-Robertson-Walker (FRW) Universe filled by
radiation fluid. We have studied the dependency on the curvature profile of the
initial mass $M_{\rm BH,i}$ of the PBHs at the time of apparent horizon
formation $t_{AH}$, and the final mass $M_{\rm BH,f}$ after the accretion
process, using an excision technique, comparing $M_{\rm BH,i}$ to previous
analytical estimations obtained using compensated PBHs model approach. The
analytical estimations are in agreement with numerical results, except for
large values of the initial perturbation amplitude, when the compensated model
is less accurate. The masses $M_{\rm BH,f}$ and $M_{\rm BH,i}$ do not depend
only on the shape around the compaction function peak, but on the full profile
of the initial curvature perturbation. We also estimate the accretion effects,
and for those PBHs with masses relevant for the dark matter abundance, with a
final mass equal to the horizon crossing mass, we find $M_{\rm BH,f}\approx 3
M_{\rm BH,i} $.
