  The spatially flat Friedman-Robertson-Walker (FRW) cosmological model with a
massless scalar field in loop quantum cosmology admits a description in terms
of a completely solvable model. This has been used to prove that: i) the
quantum bounce that replaces the big bang singularity is generic; ii) there is
an upper bound on the energy density for all states and iii) semiclassical
states at late times had to be semiclassical before the bounce. Here we
consider a family of exact solutions to the theory, corresponding to
generalized coherent Gaussian and squeezed states. We analyze the behavior of
basic physical observables and impose restrictions on the states based on
physical considerations. These turn out to be enough to select, from all the
generalized coherent states, those that behave semiclassical at late times. We
study then the properties of such states near the bounce where the most
`quantum behavior' is expected. As it turns out, the states remain sharply
peaked and semiclassical at the bounce and the dynamics is very well
approximated by the `effective theory' throughout the time evolution. We
compare the semiclassicality properties of squeezed states to those of the
Gaussian semiclassical states and conclude that the Gaussians are better
behaved. In particular, the asymmetry in the relative fluctuations before and
after the bounce are negligible, thus ruling out claims of so called `cosmic
forgetfulness'.
