Many known FU Orionis stars are projected on the sky at the peripheries of star-forming regions. Physical association is assumed, but not yet firmly established. We investigate the cases of two such stars, FU Ori and V883 Ori, seeking kinematic evidence of their membership in young clusters associated with the Orion molecular clouds. Using astrometric data from Gaia DR3, we search for consistent 2D velocities, and we also use more limited radial velocity data to assess 3D velocities. Considering +/ − 25 pc boxes centered on λ Ori and the Orion Nebula Cluster, we use the inferred velocity fields to confirm the kinematic association of FU Ori with the former, and V883 Ori with the latter.