  At present, the best model for the evolution of the cosmos requires that dark
matter make up approximately $25\%$ of the energy content of the Universe. Most
approaches to explain the microscopic nature of dark matter, to date, have
assumed its composition to be of intrinsically weakly interacting particles;
however, this need not be the case to have consistency with all extant
observations. Given decades of inconclusive evidence to support any dark matter
candidate, there is strong motivation to consider alternatives to the standard
particle scenario. One such example is macro dark matter, a class of candidates
(macros) that could interact strongly with the particles of the Standard Model,
have large masses and physical sizes, and yet behave as dark matter. Macros
that scatter completely inelastically could have altered the primordial
production of the elements, and macro charge-dependent constraints have been
obtained previously. Here we reconsider the phenomenology of inelastically
interacting macros on the abundance of primordially produced $^4\text{He}$ and
revise previous constraints by also taking into account improved measurements
of the primordial $^4\text{He}$ abundance. The constraints derived here are
limited in applicability to only leptophobic macros that have a surface
potential $V \gtrsim 0.5\,$MeV. However, an important conclusion from our
analysis is that even neutral macros would likely affect the abundance of the
light elements. Therefore, constraints on that scenario are possible and are
currently an open question.
