  In this paper we explore the interplay between intermediate-mass black holes
(IMBHs) and their nursing globular clusters (GCs), taking advantage of over
2000 Monte Carlo GC models. We find that the average density of IMBHs sphere of
influence can be uniquely connected to the host GCs luminosity and half-light
radius via a fundamental plane. We propose a statistical approach to
systematically identify potential Galactic GCs harbouring either an IMBH or a
massive subsystem comprised of stellar BHs. Our models show that the IMBH is
often bound to a stellar companion or a stellar BH, which can lead to tidal
disruption events or to low-frequency gravitational waves. We show that GCs
orbiting close to the Galactic Centre have a larger probability to witness IMBH
formation during their early evolution. These low-orbit GCs can deliver several
IMBHs into the galaxy innermost regions, with potential impact on both
electromagnetic and GW emission. We discuss potential connections between IMBHs
and SMBHs inhabiting galactic nuclei, exploring the possibility that in some
cases they share similar formation pathways.

Astrophysics of Galaxies;High Energy Astrophysical Phenomena;Solar and Stellar Astrophysics