  In this work we investigate protoneutron star properties within a modified
version of the quark coupling model (QMC) that incorporates a omega-rho
interaction plus kaon condensed matter at finite temperature. Fixed entropy and
trapped neutrinos are taken into account. Our results are compared with the
ones obtained with the GM1 parametrization of the non-linear Walecka model for
similar values of the symmetry energy slope. Contrary to GM1, within the QMC
the formation of low mass black-holes during cooling are not probable. It is
shown that the evolution of the protoneutron star may include the melting of
the kaon condensate driven by the neutrino diffusion, followed by the formation
of a second condensate after cooling. The signature of this complex proccess
could be a neutrino signal followed by a gamma ray burst. We have seen that
both models can, in general, describe very massive stars.
