Formation of Very Young Massive Clusters and implications for globular
  clusters
  How Very Young Massive star Clusters (VYMCs; also known as "starburst"
clusters), which typically are of $\gtrsim 10^4M_\odot$ and are a few Myr old,
form out of Giant Molecular Clouds is still largely an open question.
Increasingly detailed observations of young star clusters and star-forming
molecular clouds and computational studies provide clues about their formation
scenarios and the underlying physical processes involved. This chapter is
focused on reviewing the decade-long studies that attempt to computationally
reproduce the well-observed nearby VYMCs, such as the Orion Nebula Cluster,
R136 and NGC 3603 young cluster, thereby shedding light on birth conditions of
massive star clusters, in general. On this regard, focus is given on direct
N-body modeling of real-sized massive star clusters, with a monolithic
structure and undergoing residual gas expulsion, which have consistently
reproduced the observed characteristics of several VYMCs and also of young star
clusters, in general. The connection of these relatively simplified model
calculations with the structural richness of dense molecular clouds and the
complexity of hydrodynamic calculations of star cluster formation is presented
in detail. Furthermore, the connections of such VYMCs with globular clusters,
which are nearly as old as our Universe, is discussed. The chapter is concluded
by addressing long-term deeply gas-embedded (at least apparently) and
substructured systems like W3 Main. While most of the results are quoted from
existing and up-to-date literature, in an integrated fashion, several new
insights and discussions are provided.
