  We do a morphological, kinematic and chemical analysis of the disrupting
cluster UBC 274 (2.5 Gyr, $d=1778$ pc) to study its global properties. We use
HDBSCAN to obtain a new membership list up to 50 pc from its centre and up to
magnitude $G=19$ using Gaia EDR3 data. We use high resolution and high
signal-to-noise spectra to obtain atmospheric parameters of 6 giants and
subgiants, and individual abundances of 18 chemical species. The cluster has a
highly eccentric (0.93) component, tilted $\sim$10 deg with respect to the
plane of the Galaxy, which is morphologically compatible with the result of a
test-particle simulation of a disrupting cluster. Our abundance analysis shows
that the cluster has a subsolar metallicity of [Fe/H]$=-0.08\pm0.02$. Its
chemical pattern is compatible with that of Ruprecht 147, of similar age but
located closer to the Sun, with the remarkable exception of neutron-capture
elements, which present an overabundance of $[n\mathrm{/Fe]}\sim0.1$. The
cluster's elongated morphology is associated with the internal part of its
tidal tail, following the expected dynamical process of disruption. We find a
significant sign of mass segregation where the most massive stars appear 1.5
times more concentrated than other stars. The cluster's overabundance of
neutron-capture elements can be related to the metallicity dependence of the
neutron-capture yields due to the secondary nature of these elements, predicted
by some models. UBC 274 presents a high chemical homogeneity at the level of
$0.03$ dex in the sampled region of its tidal tails.
