An intravalley paleolake (more than 400 m deep) was detected along the course of Shalbatana Vallis from the evidence of shorelines and the occurrence of a few fan-delta deposits (including a Gilbert-type delta). The fronts of all the sedimentary deposits strikingly match the same topographic contours (2800 and 3000 m below the Martian datum), indicating the paleolake water levels under which they formed. Also, the corresponding shorelines are visible along the Shalbatana Vallis walls. The peculiar settings of the lake suggest that Shalbatana Vallis was impounded during its final hydrological activity and that ponding of water lasted enough time to allow the formation and evolution of the lacustrine system. Water source is uncertain, but a composite sapping mechanism is hypothesized in order to take into account the amount of water required to excavate, transport, and deposit the materials found in the deposits. Previous works and new crater counting computations indicate that the paleolake was active during the Hesperian epoch; therefore, at that time, surface conditions were different from those of modern Mars and supportive of flow and ponding of water. It is unclear whether the hydrological activity was sustained entirely by a favorable climatic regime and secondary regional factors like volcanism, impact cratering, and tectonism could have also triggered/accelerated the local groundwater activity, implying that the system could have evolved relatively independent from climatic conditions. The latter eventuality and the regional importance of this research advised against an extrapolation of its results to the overall debate about Martian climatic-geomorphological evolution.