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We present molecular line and dust continuum observations of aPlanck-detected cold cloud, G074.11+00.11. The cloud consists of a system ofcurved filaments and a central star-forming clump. The clump is associated withseveral infrared sources and H2O maser emission. We aim to determine the massdistribution and gas dynamics within the clump, to investigate if thefilamentary structure seen around the clump repeats itself on a smaller scale,and to estimate the fractions of mass contained in dense cores and filaments.The velocity distribution of pristine dense gas can be used to investigate theglobal dynamical state of the clump, the role of filamentary inflows, filamentfragmentation and core accretion. We use molecular line and continuumobservations from single dish observatories and interferometric facilities tostudy the kinematics of the region. The molecular line observations show thatthe central clump may have formed as a result of a large-scale filamentcollision. The central clump contains three compact cores. Assuming a distanceof 2.3 kpc, based on Gaia observations and a three-dimensional extinctionmethod of background stars, the mass of the central clump exceeds 700 solarmasses, which is roughly 25% of the total mass of the cloud. Our virialanalysis suggests that the central clump and all identified substructures arecollapsing. We find no evidence for small-scale filaments associated with thecores. Our observations indicate that the clump is fragmented into three coreswith masses in the range [10,50] solar masses and that all three arecollapsing. The presence of an H2O maser emission suggests active starformation. However, the CO lines show only weak signs of outflows. We suggestthat the region is young and any processes leading to star formation have justrecently begun.

Cloud G074.11+00.11: a stellar cluster in formation