  Short-period super-Earths and mini-Neptunes encircle more than $\sim50\%$ of
Sun-like stars and are relatively amenable to direct observational
characterization. Despite this, environments in which these planets accrete are
difficult to probe directly. Nevertheless, pairs of planets that are close to
orbital resonances provide a unique window into the inner regions of
protoplanetary disks, as they preserve the conditions of their formation, as
well as the early evolution of their orbital architectures. In this work, we
present a novel approach toward quantifying transit timing variations within
multi-planetary systems and examine the near-resonant dynamics of over 100
planet pairs detected by \textit{Kepler}. Using an integrable model for
first-order resonances, we find a clear transition from libration to
circulation of the resonant angle at a period ratio of $\approx 0.6\%$ wide of
exact resonance. The orbital properties of these systems indicate that they
systematically lie far away from the resonant forced equilibrium. Cumulatively
our modeling indicates that while orbital architectures shaped by strong disk
damping or tidal dissipation are inconsistent with observations, a scenario
where stochastic stirring by turbulent eddies augments the dissipative effects
of protoplanetary disks reproduces several features of the data.
