  The circumgalactic medium (CGM) is responsive to kinetic disruptions
generated by nearby astrophysical events. In this work, we study the saturation
and dissipation of turbulent hydrodynamics within the CGM through an extensive
array of 252 numerical simulations with a large parameter space. These
simulations are endowed with proper cooling mechanisms to consistently explore
the parameter space spanned by the average gas density, metallicity, and
turbulence driving strength. A dichotomy emerges in the dynamics dissipation
behaviors. Disturbances that are hot and subsonic are characterized by weak
compression and slow dissipation, resulting in density fluctuations typically
$\lesssim 10^{-2}$. Conversely, warm supersonic turbulence, marked by
significant compression shocks and subsequent rapid cooling, is associated with
substantial clumping factors $\sim 10^0-10^1$. In the supersonic cases, the
kinetic energy decay is divided into a rate-limiting phase of shock dissipation
and a comparatively swift phase of thermal dissipation, predominantly occurring
within the overdense regions. Upon turbulence driving turnoff, the strong
density contrasts decay within a relatively brief timescale of $\sim 30 -
300~{\rm Myr}$, depending on the average gas density. Dense clouds are crushed
on similar timescales of $ \sim 30 - 100 ~{\rm Myr} $, depending on turbulence
driving strength but independent from average gas density. Results of this work
also contribute a novel dataset of dissipation timescales that incorporates an
understanding of kinematics and thermodynamics in addition to the traditional
cooling rate tables, which may serve as a valuable asset for forthcoming
simulations that aim to explore gas dynamics on galactic and cosmological
scales.
