The outskirts of the Milky Way disc have been known to be warped since the late 1950s. Although various stellar populations have shown an underlying warped distribution, the relation between the age of the population and the warp they trace remains an open question. Understanding this relation may shed light on the origin of the warp which remains a puzzle to be solved. Our goal in this work is to detect the presence of the warp in the RR Lyrae (RRL) population of the Milky Way disc. We use a compilation of the three largest public catalogues of RRL stars, precise photometric distances (~5%) and Gaia DR3 proper motions to kinematically select a sample of thin disc RRL in the Galactic anticentre, where the tangential velocity best approximates the azimuthal velocity to differentiate between those that rotate (disc) and those that do not (halo). For those disc-like RRL we analyse their mean vertical height and mean vertical velocity. We show, for the first time, that RRL stars with thin disc-like kinematics trace the warp. In the anticentre direction, the RRL population reaches a minimum in mean vertical height of ~0.4kpc, with a trend systematically lower than the one found with Classical Cepheids. The kinematical signal of the RRL warp starts at R~10kpc and, rather than resembling the Cepheid's, shows a similar trend to the Red Clump population from previous works, reaching a maximum value of ~7km/s in vertical velocity. We also obtain an estimation of the pattern speed of the RRL warp with a prograde rotation of ~13+/-2km/s/kpc, compatible with results obtained from Classical Cepheids. Finally, we also obtain a vertical velocity dispersion ~17km/s, inconsistent with the kinematics of a canonical old age (>10Gyr) disc population and, instead, favouring a population dominated by intermediate-age (3-4Gyr). Our results indicate that the thin disc RRL stars are a dynamical intermediate-age tracer of the warp, opening a new window to study the dependency of the warp with stellar age in the Milky Way.