  We study the evolution of star clusters in the Galactic tidal field starting
from their birth in molecular clumps. Our model clusters form according to the
local-density-driven cluster formation model in which the stellar density
profile is steeper than that of gas. As a result, clusters resist the gas
expulsion better than predicted by earlier models.
  We vary the impact of the Galactic tidal field {\lambda}, considering
different Galactocentric distances (3-18 kpc), as well as different cluster
sizes. Our model clusters survive the gas expulsion independent of {\lambda}.
  We investigated the relation between the cluster mass at the onset of secular
evolution and their dissolution time. The model clusters formed with a high
star-formation efficiency (SFE) follow a tight mass-dependent dissolution
relation, in agreement with previous theoretical studies. However, the low-SFE
models present a shallower mass-dependent relation than high-SFE clusters, and
most dissolve before reaching 1 Gyr (cluster teenage mortality).
