  Open star clusters are the essential building blocks of the Galactic disk;
"strong chemical tagging" - the premise that all star clusters can be
reconstructed given chemistry information alone - is a driving force behind
many current and upcoming large Galactic spectroscopic surveys. In this work,
we characterize abundance patterns for 9 elements (C, N, O, Ne, Mg, Si, S, Ca,
and Fe) in open clusters (OCs) in three galaxies (m12i, m12f, and m12m) from
the Latte suite of FIRE-2 simulations to investigate if strong chemical tagging
is possible in these simulations. We select young massive (>=10^(4.6) Msun) OCs
formed in the last ~100 Myr and calculate the intra- and inter-cluster
abundance scatter for these clusters. We compare these results with analogous
calculations drawn from observations of OCs in the Milky Way. We find the
intra-cluster scatter of the observations and simulations to be comparable.
While the abundance scatter within each cluster is minimal (<0.020 dex), the
mean abundance patterns of different clusters are not unique. We also calculate
the chemical difference in intra- and inter-cluster star pairs and find it, in
general, to be so small that it is difficult to distinguish between stars drawn
from the same OC or from different OCs. Despite tracing three distinct
nucleosynthetic families (core-collapse supernovae, white dwarf supernovae, and
stellar winds), we conclude that these elemental abundances do not provide
enough discriminating information to use strong chemical tagging for reliable
OC membership.
