  We supplement recent evolutionary computations of canonical stellar models
(i.e. with inefficient core overshooting) with Z=0.0002, 0.0004, 0.0006, 0.001,
0.004, 0.008 and suitable assumptions about the original He content.
Evolutionary results have been compared with observational data in order to
properly calibrate the efficiency of the surface convection. On this basis, we
follow the evolution of stellar models in the mass range 0.6 to 11 M$_{\odot}$
from the Main Sequence (MS) until C ignition or the onset of thermal pulses,
presenting cluster isochrones covering the range of ages from 20 Myr to 20 Gyr.
To allow a comparison with evolutionary investigations appeared in the recent
literature, we computed additional sets of models which take into account
moderate core overshooting during the H burning phase. Selected predictions
constraining the cluster ages are discussed, presenting a calibration of the
difference in magnitude between the luminous MS termination and the He burning
giants in terms of the cluster age. Both evolutionary tracks and isochrones
have been made available at the URL http://gipsy.cjb.net in the ``Pisa
Evolutionary Library'' directory.
