Geomagnetic storms represent major disturbances to Earth's magnetic field. These events are caused by enhanced solar wind driving conditions such as the arrival of large outbursts of solar plasma called Coronal Mass Ejections (CMEs). On 11 May 2024, a series of CMEs coalesced to create a geomagnetic super-storm, the largest such storm since the early 2000s. This resulted in an extreme compression of the Earth's magnetic field, well inside geosynchronous orbit, exposing essential orbital infrastructure to solar wind plasma and driving the aurora as far south as the US state of Texas and northern Mexico. The Magnetospheric Multiscale (MMS) mission's position on the edge of the magnetosphere at this time allowed us to observe the energy transfer from the solar wind to the magnetosphere. From these observations, we found enhanced ion heating, atypical electron cooling, and a typical rate of energy transport as measured by the normalized reconnection rate. Together, these results indicate that kinetic processes during strongly-driven, heavy-ion-rich magnetic reconnection may impact particle heating, while having little to no effect on the overall rate of energy transfer and convection throughout the magnetosphere.