  We have studied the long-term evolution of star clusters of the solar
neighborhood, starting from their birth in gaseous clumps until their complete
dissolution in the Galactic tidal field. We have combined the
"local-density-driven cluster formation model" of Parmentier & Pfalzner (2013)
with direct N-body simulations of clusters following instantaneous gas
expulsion.
  We have studied the relation between cluster dissolution time, $t_{dis}$, and
cluster "initial" mass, $M_{init}$, defined as the cluster {mass at the end of
the dynamical response to gas expulsion (i.e. violent relaxation), when the
cluster age is 20-30 Myr}. We consider the "initial" mass to be consistent with
other works which neglect violent relaxation. The model clusters formed with a
high star formation efficiency (SFE -- i.e. gas mass fraction converted into
stars) follow a tight mass-dependent relation, in agreement with previous
theoretical studies. However, the low-SFE models present a large scatter in
both the "initial" mass and the dissolution time, and a shallower
mass-dependent relation than high-SFE clusters. Both groups differ in their
structural properties on the average. Combining two populations of clusters,
high- and low-SFE ones, with domination of the latter, yields a cluster
dissolution time for the solar neighborhood in agreement with that inferred
from observations, without any additional destructive processes such as giant
molecular cloud encounters.
  An apparent mass-independent relation may emerge for our low-SFE clusters
when we neglect low-mass clusters (as expected for extra-galactic
observations), although more simulations are needed to investigate this aspect.
