  What is the nature of a star forming clump? Observations reveal these to be
chaotic environments being modified and influenced by many physical processes.
However, numerical simulations often define these initial star forming clumps
to be idealised objects. In this paper, we define and analyse 109 star forming
clumps extracted from our previous low-mass star cluster simulations. To define
a clump, we identify all the gas in a simulation that ever becomes bound to or
accreted onto a star, then follow the gas backwards in time until it decreases
to a critical density. This gas, and its neighbouring gas, is defined as our
star forming clump. Our clumps span a mass range of $0.15 \lesssim M/$M$_\odot
\lesssim 10.2$, while the density range within each clump spans 2--4 orders of
magnitude. The gas density distribution is not smooth, indicating that it is
highly structured. The clumps are turbulent, with no coherent rotation.
Independent of the initial magnetic field strength of the parent cloud, all
clumps yield a similar range of field strengths. The clump magnetic field is
ordered, but not reflective of the initial field geometry of the parent cloud.
In general, most clump properties have a slight trend with clump mass but are
independent of (or only very weakly dependent on) the properties of the parent
cloud. We conclude that stars are born from a wide variety of environments and
there is not a single universal star forming clump.
