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The collection of planetary system properties derived from large surveys suchas Kepler provides critical constraints on planet formation and evolution.These constraints can only be applied to planet formation models, however, ifthe observational biases and selection effects are properly accounted for. Herewe show how epos, the Exoplanet Population Observation Simulator, can be usedto constrain planet formation models by comparing the Bern planet populationsynthesis models to the Kepler exoplanetary systems. We compile a series ofdiagnostics, based on occurrence rates of different classes of planets and thearchitectures of multi-planet systems, that can be used as benchmarks forfuture and current modeling efforts. Overall, we find that a model with 100seed planetary cores per protoplanetary disk provides a reasonable match tomost diagnostics. Based on these diagnostics we identify physical propertiesand processes that would result in the Bern model more closely matching theknown planetary systems. These are: moving the planet trap at the inner diskedge outward; increasing the formation efficiency of mini-Neptunes; andreducing the fraction of stars that form observable planets. We conclude withan outlook on the composition of planets in the habitable zone, and highlightthat the majority of simulated planets smaller than 1.7 Earth radii havesubstantial hydrogen atmospheres.  The software used in this paper is available online for public scrutiny athttps://github.com/GijsMulders/epos

The Exoplanet Population Observation Simulator. II -- Population Synthesis in the Era of Kepler