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The IRDC SDC335.579-0.292 (SDC335) is a massive star-forming cloud found tobe globally collapsing towards one of the most massive star forming cores inthe Galaxy. SDC335 hosts three high-mass protostellar objects at early stagesof their evolution and archival ALMA Cycle 0 data indicate the presence of atleast one molecular outflow in the region. Observations of molecular outflowsfrom massive protostellar objects allow us to estimate the accretion rates ofthe protostars as well as to assess the disruptive impact that stars have ontheir natal clouds. The aim of this work is to identify and analyse theproperties of the protostellar-driven molecular outflows within SDC335 and usethese outflows to help refine the properties of the protostars. We imaged themolecular outflows in SDC335 using new data from the ATCA of SiO and Class ICH$_3$OH maser emission (~3 arcsec) alongside observations of four COtransitions made with APEX and archival ALMA CO, $^{13}$CO (~1 arcsec), and HNCdata. We introduced a generalised argument to constrain outflow inclinationangles based on observed outflow properties. We used the properties of eachoutflow to infer the accretion rates on the protostellar sources driving themand to deduce the evolutionary characteristics of the sources. We identifythree molecular outflows in SDC335, one associated with each of the knowncompact HII regions. The outflow properties show that the SDC335 protostars arein the early stages (Class 0) of their evolution, with the potential to formstars in excess of 50 M$_{\odot}$. The measured total accretion rate onto theprotostars is $1.4(\pm 0.1) \times 10^{-3}$M$_{\odot}$ yr$^{-1}$, comparable tothe total mass infall rate toward the cloud centre on parsec scales of 2.5$(\pm1.0) \times 10^{-3}$M$_{\odot}$ yr$^{-1}$, suggesting a near-continuous flow ofmaterial from cloud to core scales. [abridged].

Continuity of accretion from clumps to Class 0 high-mass protostars in SDC335