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The discovery of merging binary black holes via the gravitational waves they radiate has kick-started one of the most exciting times to understand how high-mass single and binary stars evolve, form black holes (and other compact objects), and end up in configurations that would merge within the Hubble time to be detectable by the LIGO-Virgo-Kagra detectors. I will review the different formation channels for merging binary black holes. I will focus on the formation of these systems through various dynamical processes and present key results. In particular, I will discuss mergers with specific properties possible only via the dynamical formation channel. Finally, I will discuss some of the current outstanding uncertainties and possible avenues to improve our ability to answer them.