  Cosmological hydrodynamical simulations are studied in order to analyse
generic trends for the stellar, baryonic and halo mass assembly of low-mass
galaxies (M_* < 3 x 10^10 M_sun) as a function of their present halo mass, in
the context of the Lambda-CDM scenario and common subgrid physics schemes. We
obtain that smaller galaxies exhibit higher specific star formation rates and
higher gas fractions. Although these trends are in rough agreement with
observations, the absolute values of these quantities tend to be lower than
observed ones since z~2. The simulated galaxy stellar mass fraction increases
with halo mass, consistently with semi-empirical inferences. However, the
predicted correlation between them shows negligible variations up to high z,
while these inferences seem to indicate some evolution. The hot gas mass in z=0
halos is higher than the central galaxy mass by a factor of ~1-1.5 and this
factor increases up to ~5-7 at z~2 for the smallest galaxies. The stellar,
baryonic and halo evolutionary tracks of simulated galaxies show that smaller
galaxies tend to delay their baryonic and stellar mass assembly with respect to
the halo one. The Supernova feedback treatment included in this model plays a
key role on this behaviour albeit the trend is still weaker than the one
inferred from observations. At z>2, the overall properties of simulated
galaxies are not in large disagreement with those derived from observations.
