  We present the results of N-body simulations meant to reproduce the long-term
effects of mutually inclined exoplanets on debris disks, using the HD 202628
system as a proxy. HD 202628 is a Gyr-old solar-type star that possesses a
directly observable, narrow debris ring with a clearly defined inner edge and
non-zero eccentricity, hinting at the existence of a sculpting exoplanet. The
eccentric nature of the disk leads us to examine the effect on it over Gyr
timescales from an eccentric and inclined planet, placed on its orbit through
scattering processes. We find that, in systems with dynamical timescales akin
to that of HD 202628, a planetary companion is capable of completely tilting
the debris disk. This tilt is preserved over the Gyr age of the system.
Simulated observations of our models show that an exoplanet around HD 202628
with an inclination misalignment $\gtrsim\,10$ degrees would cause the disk to
be observably diffuse and broad, which is inconsistent with ALMA observations.
With these observations, we conclude that if there is an exoplanet shaping this
disk, it likely had a mutual inclination of less than 5 degrees with the
primordial disk. Conclusions of this work can be either applied to debris disks
appearing as narrow rings (e.g., Fomalhaut, HR 4796), or to disks that are
vertically thick at ALMA wavelengths (e.g., HD 110058).
