  The geometries of near-resonant planetary systems offer a relatively pristine
window into the initial conditions of exoplanet systems. Given that
near-resonant systems have likely experienced minimal dynamical disruptions,
the spin-orbit orientations of these systems inform the typical outcomes of
quiescent planet formation, as well as the primordial stellar obliquity
distribution. However, few measurements have been made to constrain the
spin-orbit orientations of near-resonant systems. We present a
Rossiter-McLaughlin measurement of the near-resonant warm Jupiter TOI-2202 b,
obtained using the Carnegie Planet Finder Spectrograph (PFS) on the 6.5m
Magellan Clay Telescope. This is the eighth result from the Stellar Obliquities
in Long-period Exoplanet Systems (SOLES) survey. We derive a sky-projected 2D
spin-orbit angle $\lambda=26^{+12}_{-15}$ $^{\circ}$ and a 3D spin-orbit angle
$\psi=31^{+13}_{-11}$ $^{\circ}$, finding that TOI-2202 b - the most massive
near-resonant exoplanet with a 3D spin-orbit constraint to date - likely
deviates from exact alignment with the host star's equator. Incorporating the
full census of spin-orbit measurements for near-resonant systems, we
demonstrate that the current set of near-resonant systems with period ratios
$P_2/P_1\lesssim4$ is generally consistent with a quiescent formation pathway,
with some room for low-level ($\lesssim20^{\circ}$) protoplanetary disk
misalignments or post-disk-dispersal spin-orbit excitation. Our result
constitutes the first population-wide analysis of spin-orbit geometries for
near-resonant planetary systems.
