  The intermediate mass black hole range, $10\lesssim M_{\rm
BH}^{}/M_\odot^{}\lesssim 10^{5} $, has long offered enticing possibilities for
primordial black holes (PBH), with populations in this range postulated to be
responsible for some of the black hole binary merger detected events as well as
the existence of supermassive black holes embedded at galactic centers.
However, a prominent bound derived from PBH accretion during recombination
severely restricts the mass fraction of intermediate mass PBH. We address this
problem by proposing a formation scenario in which ``primordial" black holes
form late in our cosmological history, beyond the CMB era, and bypassing this
bound. During this crucial epoch, our population of compact objects exist as
thermal balls supported by thermal pressure, which eventually cool to Fermi
balls supported by degeneracy pressure and finally collapse to PBH. Our
mechanism is a viable production method for both the mass gap LIGO-VIRGO-KAGRA
detections and the JWST observation of an early time $z>10$ supermassive black
hole. Furthermore, we present the remarkable possibility of PBH formation after
the present era, which we term \textit{future} PBH. Such a population would
evade most, if not all bounds on the PBH mass spectrum in the literature and
open up previously unthought-of possibilities. Light future PBH could form
below the Hawking evaporation threshold and convert the bulk of the matter in
the Universe into radiation.

Cosmology and Nongalactic Astrophysics;High Energy Physics - Phenomenology