  We present, for the first time, a detailed theory of high density matter
including the entire baryon octet at finite temperature, based on a fully
relativistic mean field model with a consistent treatment of exchange (Fock)
terms, using the quark-meson-coupling model (QMC). It has been already
demonstrated that the QMC equation of state is applicable in thermodynamic
scenarios in stationary and rotating isentropic proto-neutron stars, producing
results in agreement with recent observation. It is also suitable for the
simulation of the behavior following a binary neutron star merger [1];
https://compose.obspm.fr/eos/205. We develop a comprehensive demonstration of
the impact of the Fock terms in the QMC energy density functional on properties
of neutrinoless proto-neutron stars with cores containing the full hyperon
octet with constant entropy, S/A=2kB. Given the interest in the properties of
the proto-neutron star remaining after either a supernova explosion or the
merger of two neutron stars, it is vital to develop modern equations of state
at finite temperature. While much attention has been paid to relativistic
mean-field calculations at finite temperature, it is crucial to explore the
consequences of a consistent treatment of the Fock terms.
