  Magnetically arrested accretion disks (MADs) around a rapidly rotating black
hole (BH) have been proposed as a model for jetted tidal disruption events
(TDEs). However, the dynamics of strongly magnetized disks in a more realistic
simulation which can mimic the chaotic dynamics during a TDE have previously
been unexplored. Here we employ global GRMHD simulations of a pre-existing MAD
disk interacting with an injected TDE stream with impact parameter $\beta\equiv
R_t/R_p=4-7$ to investigate how strongly magnetized TDEs differ from the
standard MAD picture. We demonstrate for the first time that a MAD or semi-MAD
state can be sustained and jets powered by the BH spin are produced in a TDE.
We also demonstrate that the strength of the self-intersection shock depends on
how dense the disk is relative to the stream, or the density contrast
$f_\rho=\rho_d/\rho_s$. The jet or funnel can become significantly tilted (by
$10-30^\circ$) due to the self-intersection outflow when $f_\rho \leq 0.1$. In
models with a powerful jet and $f_\rho\leq 0.01$, the tilted jet interacts with
and ultimately tilts the disk by as much as 23 degrees from the incoming
stream. We illustrate that as $f_\rho$ increases, the tilt of the jet and disk
is expected to realign with the BH spin once $f_\rho \geq 0.1$. We illustrate
how the tilt can rapidly realign if $f_\rho$ increases rapidly and apply this
to TDEs which have shown X-ray evolution on timescales of days-weeks.
