  We analyze the formation and evolution of terrestrial-like planets around
solar-type stars in the absence of gaseous giants. In particular, we focus on
the physical and dynamical properties of those that survive in the system's
Habitable Zone (HZ). This study is based on a comparative study between N-body
simulations that include fragmentation and others that consider all collisions
as perfect mergers. We use an N-body code, presented in a previous paper, that
allows planetary fragmentation. We carry out three sets of 24 simulations for
400 Myr. Two sets are developed adopting a model that includes hit-and-run
collisions and planetary fragmentation, each one with different values of the
individual minimum mass allowed for the fragments. For the third set, we
considered that all collisions lead to perfect mergers. The systems produced in
N-body simulations with and without fragmentation are broadly similar, with
some differences. In runs with fragmentation, the formed planets have lower
masses since part it is distributed amongst collisional fragments.
Additionally, those planets presented lower eccentricities, presumably due to
dynamical friction with the generated fragments. Perfect mergers and
hit-and-run collisions are the most common outcome. Regardless of the
collisional treatment adopted, most of the planets that survive in the HZ start
the simulation beyond the snow line, having very high final water contents. The
fragments' contribution to their mass and water content is negligible. Finally,
the individual minimum mass for fragments may play an important role in the
planets' collisional history. Collisional models that incorporate fragmentation
and hit-and-run collisions lead to a more detailed description of the physical
properties of the terrestrial-like planets formed. We conclude that planetary
fragmentation is not a barrier to the formation of water worlds in the HZ.
