  Employing the TNG100 run of the IllustrisTNG project, we characterize the
environment of Low Surface Brightness Galaxies (LSBGs) across varying scales,
from their associated dark matter halos to their distribution within the
broader cosmic structure. We find no significant differences in the halo
concentration index $c_{200}$ between LSBGs and their High Surface Brightness
(HSBGs) counterparts, with LSBGs residing in halos with higher spin parameter
$\lambda$ and slightly more spherical shapes than HSBGs. LSBGs show a stronger
alignment between the dark and stellar angular momentum vectors than their high
surface brightness counterparts. The relative abundance of LSBGs within groups
and clusters displays a central deficit, hinting at potential destruction upon
reaching these core regions. Studying the density field, we find a preference
for rotation-dominated LSBGs to reside in low-density environments, while
dispersion-dominated LSBGs thrive in high-density regions where galaxy
interactions govern their evolution, an observation corroborated by our
analysis of the two-point correlation function $\xi (r)$. Our examination of
the cosmic web reveals no significant differences in the distance to the
closest large-scale structure, barring a few exceptions. This suggests a
limited impact of large-scale spatial distribution on mechanisms driving LSBG
evolution. All together, we conclude that the halo vicinity and local
environment at the scale of galaxy clusters, where mechanisms such as galaxy
mergers and tidal stripping, as well as stellar and gas accretion take place,
is the most likely environment that favour the emergence of LSBGs with
different morphologies, mostly driven by the presence or absence of important
local interaction phenomena.
