  Super Star Clusters are one of the most extreme star forming environments in
the universe, and the most massive and dense of these may be proto globular
clusters. Like individual massive stars, the earliest stages of super star
cluster evolution are deeply obscured, and therefore our knowledge about their
birth environments is currently very incomplete. However, the study of natal
super star clusters has become somewhat of a cottage industry in recent years,
and the sample of such objects has been growing rapidly with high-quality
long-wavelength data now available from a number of observatories. The natal
super star clusters identified in thermal-infrared and radio observations
represent the youngest stage of massive star cluster evolution yet observed.
Their properties appear to be similar to those of ultracompact HII regions in
the Milky Way, but scaled up in total mass and luminosity. I will overview what
we think we know about these objects based on existing observations, discuss
their relationship to ultracompact HII regions, present new models of their
spectral energy distributions based on 3-D simulations, and outline some of the
most significant gaps in our current understanding.
