  Star formation in starbursts appears to be biased toward compact clusters,
with up to 20% of all stars formed in them. Observations with HST show that
many of these clusters have luminosities (-9 > Mv > -16), UBVI colors, and
half-light radii (R_eff = ~3 pc) consistent with their being young globular
clusters. Although we know little about the long-term stability of the youngest
clusters (<20 Myr), compact clusters older than ~10 core-crossing times (20 -
40 Myr) are bound gravitationally and very likely young globulars. The present
review concentrates on recent progress achieved in dating such clusters and on
evidence that mergers of spiral galaxies can produce relatively rich subsystems
of young globulars of solar metallicity in the remnants' halos. Studies of such
subsystems suggest a scenario in which second-generation globulars form from
giant molecular clouds squeezed into collapse by the high-pressure environment
of starbursts. These bursts, often driven by mergers, may explain ongoing
cluster formation in NGC 4038/39, the young halo globular clusters found around
protoellipticals like NGC 3921 and NGC 7252, and the subpopulations of red
metal-rich globulars observed in many giant elliptical galaxies.
