  Cosmological solutions for covariant canonical gauge theories of gravity are
presented. The underlying covariant canonical transformation framework invokes
a dynamical space-time Hamiltonian consisting of the Einstein-Hilbert term plus
a quadratic Riemann tensor invariant with a fundamental dimensionless coupling
constant $g_1$. A typical time scale related to this constant, $\tau = \sqrt{8
\pi G g_1}$, is characteristic for the type of cosmological solutions: for $t
\ll \tau$ the quadratic term is dominant, the energy-momentum tensor of the
matter is not covariantly conserved, and we observe modified dynamics of matter
and space-time. On the other hand, for $t \gg \tau$, the Einstein term
dominates and the solution converges to classical cosmology. This is analyzed
for different types of matter and dark energy with a constant equation of
state. While for a radiation dominated universe solution the cosmology does not
change, we find for a dark energy universe the well known de-Sitter space.
However, we also identify a special bouncing solution (for $k=0$) which for
large times approaches the de-Sitter space again. For a dust dominated universe
(with no pressure) deviations are seen only in the early epoch. In the late
epoch, the solution asymptotically behaves like the standard dust solution.
