Gravitational waves can be gravitationally lensed, i.e. magnified and multiply-imaged, by foreground massive galaxies or galaxy clusters in much the same way as the more familiar galaxies and quasars can be lensed.  The first detection of a gravitationally lensed gravitational wave is expected in the 2020s and will be a major milestone because it will enable the first joint study of these two pillars of General Relativity, and will reveal binary stellar mass compact objects in the distant universe (redshifts of z>1) for the first time.  I will present new predictions for the rate of lensed GWs, focussing on those expected to have electromagnetic counterparts, namely binary neutron star mergers.  I will then discuss the implications of my predictions for upcoming surveys including the Vera Rubin Observatory’s Legacy Survey of Space and Time (LSST), both from the perspective of finding new gravitational lenses and identifying candidate lensed kilonovae.  Intriguingly, Rubin non-detection of a kilonova counterpart to a candidate lensed binary neutron star merger may point to the detection of a lensed binary primordial black hole.  Exciting as that would be, interpretation of candidate lensed gravitational waves in the absence of an electromagnetic counterpart is fraught with uncertainty.  In particular, I will show that the time delay between the arrival of different images of a gravitationally lensed transient such as a gravitational wave is very sensitive to the slope of the density profile of the lens.  This motivates considering how galaxy clusters are not scaled up versions of galaxies, and segues into discussing how the shape of cluster density profiles varies from their centres out to their infall regions.  I will close by showcasing Bianconi et al.’s (arXiv:2010.05920) recent investigation of how the splash back radius of clusters depends on their assembly history.