and dark matter haloes in terms of the probability distribution that a halo of virial mass $M_h$ contains $N$ galaxies of a given type, together with the spatial and velocity distribution of galaxies inside haloes. An assumed cosmology and a specified shape of the HOD then allows us to predict any galaxy clustering statistic. The HOD approach is a powerful way to interpret observed galaxy clustering measurements, essentially transforming correlation function measurements to the relationship connecting galaxies with haloes (e.g., @Zehavi:2011 [@Coupon:2012] and references therein). It is also a useful method to characterize the predictions of galaxy formation models in a concise form that allows us to quantify the galaxy-halo relation (e.g., @Zheng:2005 [@C13; @C17]). Another important application of the HOD approach is to facilitate the generation of realistic galaxy mock catalogues by populating dark matter haloes from an N-body simulation with galaxies that reproduce a particular target clustering measurement. This method has become increasingly popular due to the growing demand for such catalogues for planning for and interpreting the results from large galaxy surveys and due to its good performance and low computational cost (e.g., @Manera:2015 [@Zheng:2016]). In the standard HOD framework mass is the only halo property that 