  By performing global hydrodynamical simulations of accretion discs with
driven turbulence models, we demonstrate that elevated levels of turbulence
induce highly stochastic migration torques on low-mass companions embedded in
these discs. This scenario applies to planets migrating within
gravito-turbulent regions of protoplanetary discs as well as stars and black
holes embedded in the outskirts of active galactic nuclei (AGN) accretion
discs. When the turbulence level is low, linear Lindblad torques persists in
the background of stochastic forces and its accumulative effect can still
dominate over relatively long timescales. However, in the presence of very
stronger turbulence, classical flow patterns around the companion embedded in
the disc are disrupted, leading to significant deviations from the expectations
of classical Type I migration theory over arbitrarily long timescales. Our
findings suggest that the stochastic nature of turbulent migration can prevent
low-mass companions from monotonically settling into universal migration traps
within the traditional laminar disc framework, thus reducing the frequency of
three-body interactions and hierarchical mergers compared to previously
expected. We propose a scaling for the transition mass ratio from classical to
chaotic migration $q\propto \alpha_R$, where $\alpha_R$ is the Reynolds
viscosity stress parameter, which can be further tested and refined by
conducting extensive simulations over the relevant parameter space.
