[en] We report the detection of the 1.3 mm continuum and the molecular emission of the disks of the young triple system SR24 by analyzing ALMA (The Atacama Large Millimeter/Submillimter Array) subarcsecond archival observations. We estimate the mass of the disks (0.025 M _☉ and 4 × 10⁻⁵ M _⊕ for SR24S and SR24N, respectively) and the dynamical mass of the protostars (1.5 M _☉ and 1.1 M _☉). A kinematic model of the SR24S disk to fit its C¹⁸O (2-1) emission allows us to develop an observational method to determine the tilt of a rotating and accreting disk. We derive the size, inclination, position angle, and sense of rotation of each disk, finding that they are strongly misaligned (${108}^{\circ <!--\; ???\; -->}$) and possibly rotate in opposite directions as seen from Earth, in projection. We compare the ALMA observations with ¹²CO SMA archival observations, which are more sensitive to extended structures. We find three extended structures and estimate their masses: a molecular bridge joining the disks of the system, a molecular gas reservoir associated with SR24N, and a gas streamer associated with SR24S. Finally, we discuss the possible origin of the misaligned SR24 system, concluding that a closer inspection of the northern gas reservoir is needed to better understand it.