Flux ropes are frequently defined as bundles of solar magnetic field lines, twisting around a common axis. Formed through a combination of photospheric surface flows and magnetic reconnection, these flux ropes can act to store magnetic stresses as they build in the corona. Beyond a critical quantity of twist, flux rope eruptions can push magnetic field and plasma outward into the heliosphere as a coronal mass ejection (CME). Understanding the formation and eruption of flux ropes is critical in studying and predicting space weather phenomena. Here we present an automated methodology to identify flux ropes within magnetofrictional simulations of the coronal magnetic field, driven by observational data. With this methodology, flux rope volumes are precisely tied down to enable consistent solar-cycle length statistical descriptions of eruption rates, spatial distribution, magnetic orientation, and magnetic flux. Through modification of model parameters and driving input data we arrive at a better understanding of flux rope eruption. For Earth-directed CMEs, potential hints towards associated magnetic orientation, helicity, and flux greatly expand our ability to predict geo-effectiveness.