  The tidal torque theory (TTT) relates the origin and evolution of angular
momentum with the environment in which dark matter (DM) haloes form. The
deviations introduced by late non-linearities are commonly thought as noise in
the model. In this work, we analyze a cosmological simulation looking for
systematics on these deviations, finding that the classification of DM haloes
according to their angular momentum growth results in samples with different
internal alignment, spin parameter distribution and assembly history. Based on
this classification, we obtain that low mass haloes are embedded in denser
environments if they have acquired angular momentum below the TTT expectations
(L haloes), whereas at high masses enhanced clustering is typically associated
with higher angular momentum growths (W haloes). Additionally, we find that the
low mass signal has a weak dependence on the direction, whereas the high mass
signal is entirely due to the structure perpendicular to the angular momentum.
Finally, we study the anisotropy of the matter distribution around haloes as a
function of their mass. We find that the angular momentum direction of W (L)
haloes remains statistically perpendicular (parallel) to the surrounding
structure across the mass range
$11<\mathrm{log}(M/h^{-1}\mathrm{M}_{\odot})<14$, whereas haloes following TTT
show a "spin flip" mass consistent with previously reported values ($\sim 5
\times 10^{12}$ $h^{-1}\mathrm{M}_\odot$). Hence, whether the spin flip mass of
the deviated samples is highly shifted or straightly undefined, our results
indicate that is remarkably connected to the haloes angular momentum growth.
