  Galaxy surveys map the three-dimensional distribution of matter in the
Universe, encoding information about both the primordial cosmos and its
subsequent evolution. By comparing the angular and physical scales of features
in the galaxy distribution, we can compute the physical distance to the sample,
and thus extract the Hubble parameter, $H_0$. In this chapter, we discuss how
this is performed in practice, introducing two key ``standard rulers''. The
first, the sound horizon at recombination, leads to baryon acoustic
oscillations, and, by combining with external data from the CMB or Big Bang
Nucleosynthesis, leads to a competitive $H_0$ constraint. Information can also
be extracted from the physical scale of the horizon at matter-radiation
equality; though somewhat less constraining, this depends on very different
physics and is an important validation test of the physical model. We discuss
how both such constraints can be derived (using ``template'' and ``full-shape''
methodologies), and present a number of recent constraints from the literature,
some of which are comparable in precision to (and independent from) Planck.
Finally, we discuss future prospects for improving these constraints in the
future.
