  Very young asteroid families may record processes that accompanied their
formation in the most pristine way. This makes analysis of this special class
particularly interesting. We studied the very young Adelaide family in the
inner part of the main belt. This cluster is extremely close to the previously
known Datura family in the space of proper orbital elements and their ages
overlap. As a result, we investigated the possibility of a causal relationship
between the two families. We identified Adelaide family members in the
up-to-date catalogue of asteroids. By computing their proper orbital elements
we inferred the family structure. Backward orbital integration of selected
members allowed us to determine the age of the family. The largest fragment
(525) Adelaide, an S-type asteroid about $10$ km in size, is accompanied by 50
sub-kilometre fragments. This family is a typical example of a cratering event.
The very tiny extent in the semi-major axis minimises chances that some
significant mean motion resonances influence the dynamics of its members,
though we recognise that part of the Adelaide family is affected by weak,
three-body resonances. Weak chaos is also produced by distant encounters with
Mars. Simultaneous convergence of longitude of node for the orbits of six
selected members to that of (525) Adelaide constrains the Adelaide family age
to $536\pm 12$ kyr (formal solution). While suspiciously overlapping with the
age of the Datura family, we find it unlikely that the formation events of the
two families are causally linked. In all likelihood, the similarity of their
ages is just a coincidence.
