  According to a standard initial mass function, stars in the range 7-12 Msun
constitute ~50% (by number) of the stars more massive than ~7 Msun, but, in
spite of this, their evolutionary properties, and in particular their final
fate, are still scarcely studied. In this paper we present a detailed study of
the evolutionary properties of solar metallicity, non rotating stars in the
range 7-15 Msun, from the pre main sequence phase up to the presupernova stage
or up to an advanced stage of the thermally pulsing phase, depending on the
initial mass. We find that (1) the 7.00 Msun develops a degenerate CO core and
evolves as a classical AGB star in the sense that it does not ignite the C
burning reactions; (2) stars with the initial mass M >= 9.22 Msun end their
life as core collapse supernovae; (3) stars in the range 7.50 <= M/Msun <= 9.20
develop a degenerate ONeMg core and evolve through the thermally pulsing SAGB
phase; 4) stars in the mass range 7.50 <= M/Msun <= 8.00 end their life as
hybrid CO/ONeMg- or ONeMg- WD; (5) stars with the initial mass in the range
8.50 <= M/Msun <= 9.20 may potentially explode as electron capture supernovae.
