  We present ground-based infrared transit observations for four dynamically
interacting \textit{Kepler} planets, including Kepler-29b, Kepler-36c,
KOI-1783.01, and Kepler-177c, obtained using the Wide-field Infrared Camera on
the Hale 200" telescope at Palomar Observatory. By utilizing an engineered
diffuser and custom guiding software, we mitigate time-correlated telluric and
instrumental noise sources in these observations. We achieve an infrared
photometric precision comparable to or better than that of space-based
observatories such as the \textit{Spitzer Space Telescope}, and detect transits
with greater than 3$\sigma$ significance for all planets. For Kepler-177c
($J=13.9$) our measurement uncertainties are only $1.2\times$ the photon noise
limit and 1.9 times better than the predicted photometric precision for
\textit{Spitzer} IRAC photometry of this same target. We find that a single
transit observation obtained $4-5$ years after the end of the original
\textit{Kepler} mission can reduce dynamical mass uncertainties by as much as a
factor of three for these systems. Additionally, we combine our new
observations of KOI-1783.01 with information from the literature to confirm the
planetary nature of this system. We discuss the implications of our new mass
and radius constraints in the context of known exoplanets with low incident
fluxes, and we note that Kepler-177c may be a more massive analog to the
currently known super-puffs given its core mass (3.8$\pm0.9M_\Earth$) and large
gas-to-core ratio (2.8$\pm0.7$). Our demonstrated infrared photometric
performance opens up new avenues for ground-based observations of transiting
exoplanets previously thought to be restricted to space-based investigation.
