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We analyze the clustering of galaxies using the z=1.006 snapshot of theCosmoDC2 simulation, a high-fidelity synthetic galaxy catalog designed tovalidate analysis methods for the Large Synoptic Survey Telescope (LSST). Wepresent sub-percent measurements of the galaxy auto-correlation and galaxy-darkmatter cross correlations in Fourier space and configuration space for amagnitude-limited galaxy sample. At these levels of precision, the statisticalerrors of the measurement are comparable to the systematic effects present inthe simulation and measurement procedure; nevertheless, using a hybrid-PTmodel, we are able to model non-linear galaxy bias with 0.5% precision up toscales of $k_{\rm max}= 0.5 \ h/{\rm Mpc}$ and $r_{\rm min}= 4 \ {\rm Mpc}/h$.While the linear bias parameter is measured with 0.01% precision, other biasparameters are determined with considerably weaker constraints and sometimesbimodal posterior distributions. We compare our fiducial model with lowerdimensional models where the higher-order bias parameters are fixed at theirco-evolution values and find that leaving these parameters free providessignificant improvements in our ability to model small scale information. Wealso compare bias parameters for galaxy samples defined using differentmagnitude bands and find agreement between samples containing equal numbers ofgalaxies. Finally, we compare bias parameters between Fourier space andconfiguration space and find moderate tension between the two approaches.Although our model is often unable to fit the CosmoDC2 galaxy samples withinthe 0.1% precision of our measurements, our results suggest that the hybrid-PTmodel used in this analysis is capable of modeling non-linear galaxy biaswithin the percent level precision needed for upcoming galaxy surveys.

Perturbation theory models for LSST-era galaxy clustering: tests with sub-percent mock catalog measurements in Fourier and configuration space