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A leading theoretical expectation for the final stages of planet formation isthat disk migration should naturally drive orbits into chains of mean motionresonances (MMRs). In order to explain the dearth of MMR chains observed at Gyrages ($<1\%$), this picture requires such configurations to destabilize andscramble period ratios following disk dispersal. Strikingly, the only two knownstars with three or more planets younger than $\lesssim 100$ Myrs, HR 8799 andV1298 Tau, have been suggested to be in such MMR chains, given the orbits'near-integer period ratios. We incorporate recent transit and radial velocityobservations of the V1298 Tau system, and investigate constraints on thesystem's orbital architecture imposed by requiring dynamical stability ontimescales much shorter than the system's age. We show that the recentradial-velocity mass measurement of V1298 Tau $b$ places it within a factor oftwo of the instability limit, and that this allows us to set significantlylower limits on the eccentricity ($e_b \leq 0.17$ at $99.7\%$ confidence).Additionally, we rule out a resonant chain configuration for V1298 Tau at$\gtrsim 99\%$ confidence. Thus, if the $\sim 23$ Myr-old V1298 Tau system didform as a resonant chain, it must have undergone instability and rearrangementshortly after disk dispersal. We expect that similar stability constrainedcharacterization of future young multi-planet systems will be valuable ininforming planet formation models.

Stability Constrained Characterization of the 23 Myr-old V1298 Tau System: Do Young Planets Form in Mean Motion Resonance Chains?