Star Clusters in the Galactic tidal field, from birth to dissolution
  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).
