Proton cyclotron waves (PCWs) upstream from Mars are generated by ion–ion instabilities due to the interaction between the solar wind and the pickup protons that originate from the extended hydrogen (H) exosphere of Mars, indicating a loss of H to interplanetary space. Their occurrences and properties associated with nominal solar wind conditions have been widely studied, but relatively little is known about PCW activity under extreme solar wind conditions. In this work we characterize the upstream PCWs during the passage of solar wind stream interaction regions (SIRs) utilizing in situ observations by the Mars Atmosphere and Volatile EvolutioN spacecraft from October 2014 to August 2021. The 46 analyzed SIR events are a subset of the events that occurred in the perihelion season of Martian years 32–35. We find that the PCW occurrence rate is increased by a factor of about 1.8 during the SIR phase relative to the pre-SIR and post-SIR phases. Furthermore, the PCW activity tends to occur more frequently in the leading portion of the SIR. The PCWs detected during the SIR phase have more pronounced wave characteristics, namely larger wave amplitudes, smaller propagation angles with respect to the background magnetic field, and closer-to-circular polarization.