can potentially have important implications for interpreting galaxy clustering using the HOD framework (e.g., @Zentner:2014). Detecting galaxy assembly bias has proven challenging and controversial. Despite some studies which claim to have uncovered the existence of assembly bias in the observable Universe (e.g., @Berlind:2006 [@Yang:2006; @Cooper:2010; @Wang:2013b; @Lacerna:2014; @Hearin:2015; @Miyatake:2016; @Saito:2016]) others argue that the impact of assembly is small [@Abbas:2006; @Blanton:2007; @Tinker:2008; @Tinker:2011; @Lin:2016; @Zu:2016a; @Dvornik:2017] or that the assembly bias signal could be a result of different systematics (e.g. @Campbell:2015b [@Zu:2016b; @Zu:2017; @Busch:2017; @Sin:2017; @Tinker:2017a; @Lacerna:2018]).

This is the latest in a series of papers examining the spatial distribution of galaxies predicted by SAMs. [@C13] examined the clustering and HOD predicted by SAMS from different groups and found that the models give robust clustering predictions when the galaxies are selected by properties that scale with the halo mass (such as stellar mass). [@C15] studied how predicted galaxy properties (such as stellar mass, cold gas mass, star formation rate, and black hole mass) correlate with their host halo mass in different SAMs. [@C17] examined how the predicted HOD form evolves with redshift in SAMs. We proposed a parametric form for the evolution of the HOD fitting parameters that can be 