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Context. The physical processes driving the formation of Galactic spiral armsare still under debate. Studies using open clusters favour the description ofthe Milky Way spiral arms as long-lived structures following the classicaldensity wave theory. Current studies comparing the Gaia DR2 field starskinematic information of the Solar neighbourhood to simulations, find a betteragreement with short-lived arms with a transient behaviour. Aims. Our aim is toprovide an observational, data-driven view of the Milky Way spiral structureand its dynamics using open clusters as the main tracers, and to contrast itwith simulation-based approaches. We use the most complete catalogue of MilkyWay open clusters, with astrometric Gaia EDR3 updated parameters, estimatedastrophysical information and radial velocities, to re-visit the nature of thespiral pattern of the Galaxy. Methods. We use a Gaussian mixture model todetect overdensities of open clusters younger than 30 Myr that correspond tothe Perseus, Local, Sagittarius and Scutum spiral arms, respectively. We usethe birthplaces of the open cluster population younger than 80 Myr to trace theevolution of the different spiral arms and compute their pattern speed. Weanalyse the age distribution of the open clusters across the spiral arms toexplore the differences in the rotational velocity of stars and spiral arms.Results. We are able to increase the range in Galactic azimuth wherepresent-day spiral arms are described, better estimating its parameters byadding 264 young open clusters to the 84 high-mass star-forming regions used sofar, thus increasing by a 314% the number of tracers. We use the evolution ofthe open clusters from their birth positions to find that spiral arms nearlyco-rotate with field stars at any given radius, discarding a common spiralpattern speed for the spiral arms explored. [abridged]

On the Milky Way spiral arms from open clusters in Gaia EDR3